1,476 research outputs found
Fabrication of 2D Material Based NEMS Resonators
2D materials such as graphene, MoS2 and phosphorene are promising candidates for resonating mechanical sensors due to excellent tunable electrical/- mechanical properties, low masses, and maximal surface to volume ratios. Mechanical resonators based on supsended graphene have been realized. - CVD graphene wet-transferred onto 10x10 mm Si/SiO2 chips with Au electrodes - Graphene patterned in O2 plasma with a resist mask - Graphene is released by etching SiO2 in BHF and critical point dryin
The Case for the Dual Halo of the Milky Way
Carollo et al. have recently resolved the stellar population of the Milky Way
halo into at least two distinct components, an inner halo and an outer halo.
This result has been criticized by Schoenrich et al., who claim that the
retrograde signature associated with the outer halo is due to the adoption of
faulty distances. We refute this claim, and demonstrate that the Schoenrich et
al. photometric distances are themselves flawed because they adopted an
incorrect main-sequence absolute magnitude relationship from the work of
Ivezi\'c et al. When compared to the recommended relation from Ivezi\'c et al.,
which is tied to a Milky Way globular cluster distance scale and accounts for
age and metallicity effects, the relation adopted by Schoenrich et al. yields
up to 18% shorter distances for stars near the main-sequence turnoff (TO). Use
of the correct relationship yields agreement between the distances assigned by
Carollo et al. and Ivezi\'{c} et al. for low-metallicity dwarfs to within
6-10%. Schoenrich et al. also point out that intermediate-gravity stars (3.5 <=
log g <= 4.0) with colors redder than the TO region are likely misclassified,
with which we concur. We implement a new procedure to reassign luminosity
classifications for the TO stars that require it. New derivations of the
rotational behavior demonstrate that the retrograde signature and high velocity
dispersion of the outer-halo population remains. We summarize additional lines
of evidence for a dual halo, including a test of the retrograde signature based
on proper motions alone, and conclude that the preponderance of evidence
strongly rejects the single-halo interpretation.Comment: 46 pages, 2 tables, 15 figures, Accepted for publication in the
Astrophysical Journa
Virial Sequences for Thick Discs and Haloes: Flattening and Global Anisotropy
The virial theorem prescribes the ratio of the globally-averaged equatorial
to vertical velocity dispersion of a tracer population in spherical and
flattened dark haloes. This gives sequences of physical models in the plane of
global anisotropy and flattening. The tracer may have any density, though there
are particularly simple results for power-laws and exponentials. We prove the
flattening theorem: for a spheroidally stratified tracer density with axis
ratio q in a dark density potential with axis ratio g, the ratio of globally
averaged equatorial to vertical velocity dispersion depends only on q/g. As the
stellar halo density and velocity dispersion of the Milky Way are accessible to
observations, this provides a new method for measuring the flattening of the
dark matter. If the kinematics of the local halo subdwarfs are representative,
then the Milky Way's dark halo is oblate with a flattening in the potential of
g ~ 0.85, corresponding to a flattening in the dark matter density of ~ 0.7.
The fractional pressure excess for power-law populations is roughly
proportional to both the ellipticity and the fall-off exponent. Given the same
pressure excess, if the density profile of one stellar population declines more
quickly than that of another, then it must be rounder. This implies that the
dual halo structure claimed by Carollo et al. (2007) for the Galaxy, a flatter
inner halo and a rounder outer halo, is inconsistent with the virial theorem.
For the thick disc, we provide formulae for the virial sequences of
double-exponential discs in logarithmic and Navarro-Frenk-White (NFW) haloes.
There are good matches to the observational data on the flattening and
anisotropy of the thick disc if the thin disc is exponential with a short
scalelength ~ 2.6 kpc and normalisation of 56 solar masses per square parsec,
together with a logarithmic dark halo.Comment: MNRAS, submitted, 13 pages, 7 figures, small changes to made to
correspond to final accepted versio
Binary Contamination in the SEGUE sample: Effects on SSPP Determinations of Stellar Atmospheric Parameters
Using numerical modeling and a grid of synthetic spectra, we examine the
effects that unresolved binaries have on the determination of various stellar
atmospheric parameters for SEGUE targets measured using the SEGUE Stellar
Parameter Pipeline (SSPP). To model undetected binaries that may be in the
SEGUE sample, we use a variety of mass distributions for the primary and
secondary stars in conjunction with empirically determined relationships for
orbital parameters to determine the fraction of G-K dwarf stars, as defined by
SDSS color cuts, that will be blended with a secondary companion. We focus on
the G-K dwarf sample in SEGUE as it records the history of chemical enrichment
in our galaxy. To determine the effect of the secondary on the spectroscopic
parameters, we synthesize a grid of model spectra from 3275 to 7850 K (~0.1 to
1.0 \msun) and [Fe/H]=-0.5 to -2.5 from MARCS model atmospheres using
TurboSpectrum. We analyze both "infinite" signal-to-noise ratio (S/N) models
and degraded versions, at median S/N of 50, 25 and 10. By running individual
and combined spectra (representing the binaries) through the SSPP, we determine
that ~10% of the blended G-K dwarf pairs with S/N>=25 will have their
atmospheric parameter determinations, in particular temperature and
metallicity, noticeably affected by the presence of an undetected secondary. To
account for the additional uncertainty from binary contamination at a S/N~10,
uncertainties of ~140 K and ~0.17 dex in [Fe/H] must be added in quadrature to
the published uncertainties of the SSPP. (Abridged)Comment: 68 pages, 20 figures, 9 table
Primary Pneumocystis Infection in Infants Hospitalized with Acute Respiratory Tract Infection
Primary P. jirovecii infection may appear as a self-limiting upper respiratory tract infection in infants
On the alleged duality of the Galactic halo
We examine the kinematics of the Galactic halo based on SDSS/SEGUE data by
Carollo et al. (2007, 2010). We find that their claims of a counter-rotating
halo are the result of substantial biases in distance estimates (of order 50%):
the claimed retrograde component, which makes up only a tiny fraction of the
entire sample, prone to contaminations, is identified as the tail of distance
overestimates. The strong overestimates also result in a lift in the vertical
velocity component, which explains the large altitudes those objects were
claimed to reach. Errors are worst for the lowest metallicity stars, which
explains the metal-poor nature of the artificial component. We also argue that
measurement errors were not properly accounted for and that the use of Gaussian
fitting on intrinsically non-Gaussian Galactic components invokes the
identification of components that are distorted or even artificial. Our
evaluation of the data leads to a revision of the estimated velocity ellipsoids
and does not yield any reliable evidence for a counterrotating halo component.
If a distinct counterrotating halo component exists it must be far weaker than
claimed by Carollo et al. Finally we note that their revised analysis presented
in Beers et al. (2011) does not alleviate our main concerns.Comment: 17 pages, 12 figures, submitted to MNRA
Dark Matter Angular Momentum Profile from the Jeans Equation
Cosmological simulations of dark matter structures have shown that the
equilibrated dark matter structures have a fairly small angular momentum. It
appears from these N-body simulations that the radial profile of the angular
momentum has an almost universal behavior, even if the different dark matter
structures have experienced very different formation and merger histories. We
suggest a perturbed Jeans equation, which includes a rotational term. This is
done under a reasonable assumed form of the change in the distribution
function. By conjecturing that the (new) subdominant rotation term must be
proportional to the (old) dominant mass term, we find a clear connection, which
is in rather good agreement with the results of recent high resolution
simulations. We also present a new connection between the radial profiles of
the angular momentum and the velocity anisotropy, which is also in fair
agreement with numerical findings. Finally we show how the spin parameter
increases as a function of radius.Comment: 9 pages, 10 figures, accepted for publication in ApJ, Added
reference
Insight Into the Formation of the Milky Way Through Cold Halo Substructure. I. The ECHOS of Milky Way Formation
We identify ten -- seven for the first time -- elements of cold halo
substructure (ECHOS) in the volume within 17.5 kpc of the Sun in the inner halo
of the Milky Way. Our result is based on the observed spatial and radial
velocity distribution of metal-poor main sequence turnoff (MPMSTO) stars in 137
Sloan Extension for Galactic Understanding and Exploration (SEGUE) lines of
sight. We point out that the observed radial velocity distribution is
consistent with a smooth stellar component of the Milky Way's inner halo
overall, but disagrees significantly at the radial velocities that correspond
to our detections. We show that all of our detections are statistically
significant and that we expect no false positives. We also use our detections
and completeness estimates to infer a formal upper limit of 0.34 +/- 0.02 on
the fraction of the MPMSTO population in the inner halo that belong to ECHOS.
Our detections and completeness calculations suggest that there is a
significant population of low fractional overdensity ECHOS in the inner halo,
and we predict that 1/3 of the inner halo (by volume) harbors ECHOS with MPMSTO
star number densities n ~ 15 kpc^-3. ECHOS are likely older than known surface
brightness substructure, so our detections provide us with a direct measure of
the accretion history of the Milky Way in a region and time interval that has
yet to be fully explored. In concert with previous studies, our result suggests
that the level of merger activity has been roughly constant over the past few
Gyr and that there has been no accretion of single stellar systems more massive
than a few percent of a Milky Way mass in that interval. (abridged)Comment: 47 pages, 23 figures, and 6 tables in emulaetapj format; accepted for
publication in Ap
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